By E. N. Parker (auth.), V. Bumba, J. Kleczek (eds.)
Our first try to set up a Symposium on sun job was once made on the lAO normal meeting in Brighton 1970. There, on the consultation of fee 10, we proposed to prepare a Symposium which might tension the observational features of sunlight task. It used to be our desire that this kind of Symposium may well stimulate reviews of these very important difficulties in sun physics which for a very long time have been missed in total clinical dialogue. even if a provisional date for the Symposium used to be then made up our minds, it didn't happen to prevent overlapping with different lAO actions. on the consultation of fee 10 in Sydney -on the party of the XVth lAO common meeting in 1973 -we repeated our notion and forwarded the invitation of the Czechoslovak Academy of Sciences to arrange the Symposium in Prague. either have been approved. throughout the discussions concerning the programme of the Symposium -enthusiastically promoted by means of the past due president of fee 10, Prof. okay. O. Kiepenheuer -it was once determined to alter a little its topic. The theoreti cal difficulties have been under pressure and the vast majority of the medical Organizing Committee agreed to not care for short-lived phenomena of the sun job or with person energetic areas. Symposium No. seventy one was once held in Prague from August 25 to August 29, 1975. Its Organizing Committee consisted of V. Bumba (Chairman), W. Deinzer, R. G. Giovanelli, R. Howard, okay. O. Kiepenheuer, M. Kopecky, T. Krause, M. Kuperus, G.
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Our first try to manage a Symposium on sun task used to be made on the lAO common meeting in Brighton 1970. There, on the consultation of fee 10, we proposed to prepare a Symposium which might pressure the observational features of sunlight job. It used to be our wish that the sort of Symposium may stimulate reviews of these very important difficulties in sun physics which for a very long time have been ignored in total clinical dialogue.
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Extra resources for Basic Mechanisms of Solar Activity
5% of the rotational velocity. Poleward of 50° the errors were a little larger, but rarely greater than 25 m s-1. The number of points involved in each independent slope determination was generally greater than 600 for the equatorial latitudes, around 400 at 30°, and down to about 30 at 70°. The slope of each 5° latitude zone gives directly the average rotational velocity of that zone in km s-1. The solution in each zone is independent of the others; no points are included in more than one zone.
Meanwhile the study of the third possibilitythe convection mode - was started by Durney and Skumanich (1968), and Dumey (1968a, b). Then Busse (1970), Durney (1970), and Yoshimura and Kato (1971) found in succession that the convective modes that are most easily excited by the superadiabatic gradient in the convection zone, in other words which have the greatest growth rate and lowest critical Rayleigh number, can actually excite and maintain the equatorial acceleration. The convective modes with smaller growth rates can accelerate the higher latitudes and not necessarily the equator (Yoshimura and Kato, 1971; Yoshimura, 1972a).
Thus the velocity field considered after this step is the velocity field referenced to the central meridian region. The next step is to convert negative values of sin L to positive sin L, and for those negative sin L points the signs of the velocity signals are reversed. This has the effect of a 180° rotation about the origin in the plane of the V - sin L plot of the points with negative sin L. ) From this array of points, a slope is determined, assuming that Vm APPROACH / w / / / / SIN L E RECEDE Fig.